Examples of using Protoplanetary in English and their translations into Russian
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It's a protoplanetary system.
A parallel 3D code for simulation of galaxies and protoplanetary discs is developed.
The oldest protoplanetary disk yet discovered is 25 million years old.
As a result,they are several times more massive than in the inner part of the protoplanetary disk.
The protoplanetary disk is an accretion disk that feeds the central star.
People also translate
The star Beta Pictoris is known to have a large disk of gas anddust, possibly a protoplanetary disk.
Protoplanetary disks have been observed around several young stars in our galaxy.
They are then thought to have migrated inward due to interactions with the remains of the protoplanetary disk.
Protoplanetary disks have been observed around a very high fraction of stars in young star clusters.
Westbrook Nebula(CRL 618)is an aspherical protoplanetary nebula which is located in the constellation Auriga.
It is thought that the active magnetic fields and strong solar wind of Alfvén waves of T Tauri stars are one means by which angular momentum gets transferred from the star to the protoplanetary disc.
Later, the star forms a protoplanetary disk in which the processes of planet formation definitively end.
Under certain circumstances the disk,which can now be called protoplanetary, may give birth to a planetary system.
The Boomerang Nebula is a protoplanetary nebula located 5,000 light-years away from Earth in the constellation Centaurus.
Optical telescopes are used to look at planets, stars, galaxies,planetary nebulae and protoplanetary disks, amongst many other things.
The protoplanetary disk may also be considered an accretion disk for the star itself, because gases or other material may be falling from the inner edge of the disk onto the surface of the star.
However, recent results suggest that this object is a young star surrounded by a protoplanetary disk, at a distance of about 900 light-years away.
It has been shown that libration centers could occur prior to the formation of the bodies, when the redistribution of gaseous-dust grains occurred in protoplanetary rings.
A protoplanet is a large planetary embryo that originated within a protoplanetary disc and has undergone internal melting to produce a differentiated interior.
In the present paper, the early evolution of the Solar System with regard to the process of the formation andmass growth of small bodies in protoplanetary rings is considered.
A Sun-like star usually takes approximately 1 million years to form, with the protoplanetary disk evolving into a planetary system over the next 10-100 million years.
In this model giant planet formation is divided into two stages: a accretion of a core of approximately 10 M⊕ andb accretion of gas from the protoplanetary disk.
According to the calculations of astrophysicists at the stage of separation of the protoplanetary disk the temperature of protosolar nebula exceeded several thousand degrees.
It is assumed that when the Sun lit up, the"solar wind" blew out hydrogen, helium andother light elements from the inner zone of the protoplanetary disk to the periphery.
Roughly half of T Tauri stars have circumstellar disks,which in this case are called protoplanetary discs because they are probably the progenitors of planetary systems like the solar system.
The Titan atmosphere is characterized by the absence of heavy noble gases(Xe and Kr),as their clathrates could be formed in the protoplanetary disc only at Т 60К.
Various simulations have demonstrated that the merger of embryos in the inner part of the protoplanetary disk leads to the formation of a few Earth-sized bodies.
Old theories were unable to explain how their cores could form fast enough to accumulate significant amounts of gas from the quickly disappearing protoplanetary disk.
During the formation of planetary systems, dynamical friction between the protoplanet and the protoplanetary disk causes energy to be transferred from the protoplanet to the disk.
It proposes the migration of the giant planets from an initial compact configuration into their present positions,long after the dissipation of the initial protoplanetary disk.